adsabs/AstroCLIMB huggingface dataset:
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: Properties of the OB-stars in Leo A. ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩ is plotted versus spectral type for early-type (O-B3) stars in our sample. The spectroscopically derived ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩ are indicated by the solid markers, while the photometrically derived ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩ are the fainter bigger markers. The O-stars in Leo A are blue circles, the B-stars are purple circles, and the Be stars are purple squares. We compare our stars (χ 2 ≤ 100) with SMC results and Sextans A late-type O stars. For the SMC O-stars, we fit a best line to the V type stars in Massey et al. (2009; leftmost black dashed line, M09). For the B-type stars, we plot the O V and B V spectral types to the ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩ scale derived by Dufton et al. (2019; dashed line, D19). We also plot the fit to the Be stars in the SMC from Dunstall et al. (2011; dotted line, D11). Furthermore, we plot the two late-type O stars observed by Telford et al. (2021b; dark green, T21) and Camacho et al. (2016; light green, C16) in Sextans A, for which there is a ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩ measurement for the spectral type.
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: The figure shows a direct comparison between the parameters derived from the BEAST using the different available evolutionary models. The left panels compare the MIST models with v/vcrit = 0.4 (MR) and v/vcrit = 0.0 (MNR). The right panels compare the MIST models with v/vcrit = 0.4 (MR) to the PARSEC models (P). We plot the values for the stars in both our spectroscopic and photometric sample. The top two panels compare ﹩\mathrm{log}({T}_{\mathrm{eff}})﹩. The second two panels compare the ﹩\mathrm{log}(g)﹩. The third two panels compare M ini. The fourth panels compare ﹩\mathrm{log}(L/{L}_{\odot })﹩. The fifth panels compare ﹩\mathrm{log}(A)﹩. The bottom panels compare the A V. Stars with χ 2 < 20 for both fits are pink (good fits), stars with χ 2 > 80 in either fit are cyan (poor fits), and all other stars are purple (decent fits).
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: a) Quenched fraction of the Horizon-AGN group/cluster galaxies as a function of the halo-to-stellar mass ratio. The red line is the quenched fraction of more ancient infaller galaxies, and the blue line is that of more recent infaller galaxies. The shaded areas show 95% confidence intervals of the estimated quenched fractions. The markers and the error bars are the same as the lines and the shades but have a low number of samples (N gal ≤ 50). The black dashed line at ﹩\mathrm{log}({M}_{\mathrm{halo}}/{M}_{* })=2.75﹩ indicates the arbitrary demarcation where the trend is reversed. (b) The results of τ as a function of the halo-to-stellar mass ratio for the same galaxies. The color code and detailed format are the same as in (a).
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Residual values of τ (cluster galaxies – field galaxies) for different host mass bins, color-coded according to stellar mass bins in the same manner as illustrated in Figure 5. The median value with its standard error of each bin is shown as a shaded line. A small absolute value of Δτ indicates that the environmental effect on the SFH is negligible, while a negative value indicates the existence of the suppression of star formation by environmental effects.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption:  e-folding timescale as a function of the halo-to-stellar mass ratio. Each panel shows the position on the two-dimensional phase-space diagram. The projected distance (r proj) and line-of-sight velocity (v LOS) of galaxies are measured from 300 random lines of sight. The gray dashed lines and shades show the median values and their 16th–84th percentile uncertainties, and the black solid lines show the best fits to them. The bins with less than 300 projected galaxies are not displayed. The fitting parameters in Equation (6) are given in each panel. A relatively more robust region of the cluster is roughly marked by the thick box that includes 9 panels.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Transition epoch for the Horizon-AGN satellite galaxies in a bubble chart. The horizontal axis is the host halo mass, and the vertical axis is the stellar mass of satellite galaxies. The redder color means an earlier transition, and the bluer color means a later transition (color scales at the bottom). We set the size of bubbles based on the distributional uncertainties of transition epochs. Larger symbol size indicates that the transition clearly exists, whereas a small size indicates that there is no transition. The size indicators are shown in the left inset, and we color-coded only bins that exhibited errors smaller than 0.75 Gyr. The black dashed line is a guideline that distinguishes the reliability of the existence of the transition epoch. The top and right panels show numbers of halos and galaxies shown in Figure 2.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: The residual values of τ as a function of the host mass, as in Figure 6 but divided into different TSI bins. From left to right, the TSIs of subsamples have been increased. The color code is similar to the codes shown in Figures 5 and 6 (the red and blue colors denote massive and less massive member galaxies, respectively).
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Procedure to determine the transition epoch. We generate two mock SFHs with different τ considering their intrinsic noise. The red and blue lines show the mock SFHs of cluster and field galaxies, respectively. (a) Mean SFH of both samples. (b) Cumulative SFHs. (c) Residuals of the two cumulative SFHs. The gray vertical lines in (a) show all the crossing points that could be misidentified as the transition epoch. The black dashed line shows the determined transition epoch, corresponding to the maximum point of the residual.
Paper: Constraining Sterile Neutrino Dark Matter in the Milky Way Halo with Swift-XRT
Authors: Dominic Sicilian, Dannell Lopez, Massimo Moscetti, Esra Bulbul, Nico Cappelluti
Figure caption: Spectra and best-fit models for the total PSE (top) and FOV (bottom) data sets.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Mean SFHs of the Horizon-AGN galaxies of different masses in the same manner as Figure 3.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Summary of best-fit model streams in various halos. Leftmost panels: ﹩-\mathrm{ln}{ \mathcal L }﹩ for all model streams initiated with ﹩{v}_{{\phi }_{1}}﹩ = 150–750 km s−1 in increments of 10 km s−1 and ﹩{v}_{{\phi }_{2}}﹩ = 20–120 km s−1 in increments of 2.5 km s−1 evolved for 6 Gyr in five different dark matter halos. The Jacobi radius cut has been applied in all panels (see Section 3.3). All M 200 values are listed in units of 1012 M ⊙. The gray stars mark the combination of orbital parameters (﹩{v}_{{\phi }_{1}}﹩,﹩{v}_{{\phi }_{2}}﹩) that produced the best-fit model stream in each halo. Dark colors indicate pockets of best-fit solutions (see color bar in Figure 4). Blank spaces in the left parts of the panels indicate orbits for which the model stream did not cover the extent of the data after the Jacobi cut. Middle left panels: Visualization of the best-fit model stream in (ϕ 1, ϕ 2) space in each halo after the Jacobi radius cut, colored by the radial velocity along the stream in Cen A’s rest frame (see colorbar in Figure 5). For Halo 1 (top), the model stream does not cover the extent of the data for any orbit after the Jacobi cut, so we show an example of an orbit with (﹩{v}_{{\phi }_{1}}﹩,﹩{v}_{{\phi }_{2}}﹩) = (150,20) km s−1. The black points show the 13 control data points (x  n ), and the gray points, (y  n ), show the model stream center points at the ϕ 1 location of the control data (note that these are hard to see when the control data points overlap well with the center points of the simulated stream). The black arrows indicate the direction of motion of each model stream. Middle right panels: The 3D position of Dw3 with respect to Cen A’s center as a function of time. Rightmost panels: The best-fit model streams colored by radial velocity in Cen A’s rest frame and presented in ICRS coordinates, overplotted on the Cen A image data. The white arrows indicate the direction of motion for each model stream.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Comparison between two streams evolved in a high-mass (left) and in a low-mass (right) halo. Top left: model stream evolved for 6 Gyr in fiducial halo (colored by radial velocity in Cen A’s rest frame) and progenitor orbit (black line) projected in x and z galactic coordinates in kpc, where Cen A is located at (x, z) = (0,0). The progenitor has an initial mass of 108 M ⊙. Top right: Model stream evolved for 12 Gyr in a halo mass scaled down by a factor of four as compared to the fiducial halo. The teal line shows the orbit of the progenitor. The progenitor mass in the right panel is also scaled down by a factor of four, and its orbital velocity is scaled down by a factor of two. The two streams have identical morphologies but very different radial velocities. Bottom left: The model stream’s 3D galactocentric distance with respect to Cen A’s center as a function of time. Bottom right: Same as bottom left, but now for the progenitor with a fourth of the mass and half of the orbital velocity. Note how the tidal radius, pericenter, and apocenter distances are identical in the two cases.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Top: ﹩-\mathrm{ln}{ \mathcal L }﹩ vs. the progenitor’s line-of-sight distance with respect to Cen A for model streams evolved for 6 Gyr in the fiducial potential with fixed radial velocity, progenitor mass, and fixed (﹩{v}_{{\phi }_{1}},{v}_{{\phi }_{2}},{v}_{r}﹩) = (460, 50, −181.4) km s−1 from the best-fit model stream presented in Figure 5. There are two clear minima (best fits), located in front of (A: d = −76.0 kpc) and behind (B: d = 76.0 kpc) Cen A (which is at 3.8 Mpc). Middle: Visualization of the model streams in ICRS coordinates from the best fit in front of (A: left) and behind (B: right) Cen A overplotted on the Cen A image data and colored by the radial velocity in Cen A’s rest frame. Note how the radial velocities flip direction in the two cases. Bottom: same two model streams, but now colored by distance along the stream with respect to Cen A. The distance gradients in the southern part of the model streams are closer to us than the northern part in both cases.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Left: Prediction of the technically observable radial velocity gradients for each of the best-fit streams in each of the eight halos in which the stream could be well-fit after applying the Jacobi criterion. All M 200 values are listed in units of 1012 M ⊙. The radial velocities are evaluated at the ϕ 1 locations of the 13 control data points, x  n  (see dots), for each best-fit model stream. The best-fit model streams in the more massive halos have steeper velocity gradients. Right: Same as the left panel, but now for the line-of-sight distance gradient with respect to Cen A along each best-fit stream in each of the eight halos. The best-fit model streams in the more massive halos have shallower distance gradients along the streams.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: The best fit to the three control data points of the “second stream” (SS) in Cen A’s halo evolved in the fiducial potential integrated for 6 Gyr. We fix the radial velocity to 110 km s−1 with respect to Cen A’s rest frame and find that (﹩{v}_{{\psi }_{1}},{v}_{{\psi }_{2}}﹩) = (180,74) km s−1 minimizes ﹩-\mathrm{ln}{ \mathcal L }﹩ to be 1.99. Upper panels: ICRS projection of the best-fit simulated stream overplotted on the Cen A image data colored by the radial velocity in Cen A’s rest frame (left) and the distance along the stream with respect to Cen A’s distance (right). Bottom left: the best-fit stream visualized in (ψ 1, ψ 2) space. The red points are the three control data points. The gray points are the center points of the simulated stream evaluated at the ψ 1 position of the control data points. Bottom right: galactocentric 3D position of the simulated progenitor as a function of time.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Comparison between the best-fit model stream evolved with the Fardal et al. (2015) mock stream generator (top) and the GCD+ (Kawata & Gibson 2003) N-body follow-up (bottom). Both runs are shown in galactocentric coordinates centered on Cen A at (x, y, z) = (0,0,0), and Dw3 was evolved for 6 Gyr in the fiducial potential in both cases. Top panels: Black particles show the stars in the model stream, and the white star marks the progenitor position at present day. Bottom panels: Blue particles show the extended dark matter, and the inferno color map shows the stars. The Dw3 remnant is visible as an overdensity of stars. The stellar component of both the model stream (top) and the N-body stream (bottom) look very similar.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Values of R  s  and T 9 for different core masses that fulfill Equations (52) and (53) and the corresponding equations for Kramers’ bound-free opacities; see Appendix B.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Dependence of the density of the shell as a function of the mass of the core compared with other key densities of our toy model. Thick lines indicate the relations obtained for Thomson scattering, while thin lines depict the same relations for a Kramers’ bound-free opacity.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Schematic description of the evolution of the luminosity l(r) around the burning shell for a core with generic luminosity L  c . Note that r − and r + indicate the position of the inner and upper boundaries of the burning shell, and L  s  indicates the total energy per unit time generated in the burning shell.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Envelope integration for different values of ﹩{\mathbb{C}}﹩ and y +, for t + = 0.75 and for a Kramers’ opacity.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Evolution of the core mass M  c , shell radius R  s , and stellar radius of three full evolutionary sequences with initial masses 3 M ⊙, 5 M ⊙, and 10 M ⊙ (Z = 0.02).
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Main structural parts of a low-mass red giant.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Evolution of the radius of a 1M ⊙ model (Z = 0.02) as a function of the mass of the He core.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Top: accretion luminosity as a function of stellar luminosity. Bottom: mass accretion rate as a function of stellar mass. Black stars are the results of the Chamaeleon I survey of CTTSs from Manara et al. (2019). For this work, we plot with black dashed lines the error bars only for VW Cha. The black filled circle corresponds to the mass accretion rate computed by using the accretion luminosity from Manara et al. (2019) and stellar parameters from Daemgen et al. (2013), and error bars are shown with black dashed lines. The linear fit is taken from Fiorellino et al. (2021). Colored filled circles show the results of this work, and different colors correspond to different epochs as in Figure 8.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Accretion luminosity and mass accretion rate as a function of time.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Absolute veiling measurements.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Relative escape fractions as a function of redshift (top), M UV (bottom left), and demagnified stellar mass (bottom right). The orange points with error bars represent individual galaxies in which we have obtained flux measurements of more than 1σ significance in the LyC images (tentative detections), while 1σ upper limits for the remainder of the sample are shown by solid blue and orange triangles (which are nondetections) for high-asymmetry (A ≥ 0.35; mergers) and low-asymmetry (A < 0.35; non-merger) systems. The properties of these individual measurements are detailed in Table 2. Lighter blue triangles show the results of the stacking procedures as detailed in Table 3. Empty arrows show stacked results from the literature spanning the entire redshift range of our sample (Steidel et al. 2001; Shapley et al. 2006; Iwata et al. 2009; Boutsia et al. 2011; Grazian et al. 2017; Rutkowski et al. 2017; Marchi et al. 2018; Steidel et al. 2018; Fletcher et al. 2019; Smith et al. 2020).
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Example postage stamp cutouts and stacked images for objects in the HST UVIS F275W band in the A0370 cluster. The top row shows the F275W band cutouts representing the LyC at λ rest ≤ 912 Å. The HST ACS F606W cutouts in the bottom row depict the nonionizing flux at λ rest ≈ 1500 Å. The rightmost column shows the final stacked image, while all other columns are individual galaxies included in the stack. In total, 19 galaxies are included in the stack. As described in the text, we investigate various methods of stacking, including different centers and neighbor removal, with one example shown here. All images are shown prior to cleaning; however, the final measurements are taken after the removal of neighboring objects and contaminants. Postage stamps are 4″ along each side.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Mosaic showing 40 out of our 42 sources with valid asymmetry measurements listed with their ID and asymmetry values. Sources 3266 and 4213 are not included because their low S/N makes CAS measurements impossible. The asymmetry value for each galaxy is located in the top left corner, while the source identification and band used for the measurement are located at the bottom left corner. Each source image shows the Petrosian region (1.5R P) used to measure the main term of Equation (4) in each viridis color map. The gray area was smoothed with a Gaussian kernel for visualization purposes. The background term of the asymmetry, A BG, is measured with the original pixel values that are beyond the Petrosian region away from any other galaxy. The values of the magnification for each galaxy are listed in Table 2.